HXMT的空间环境本底计算

硬X射线调制望远镜(HXMT)是一颗宽波段X射线(1～250 keV)天文卫星,其核心载荷高能X射线望远镜(HE)工作于硬X射线能区(20～250 keV),致力于实现硬X射线的高灵敏度巡天观测,描绘硬X射线天图,并对特殊天体作高灵敏度定点观测.为了获得高灵敏度,必须有效地抑制本底.本底主要是由轨道环境中的粒子(γ射线、质子、电子、中子)与探测器相互作用产生的.本文结合大量的描述近地空间本底的文献和最新的实测数据,整理出一套自洽的近地空间本底粒子的数据和公式,便于应用.并通过Geant 4软件模拟计算给出了HXMT的本底及本底随时间和轨道的变化.      

基于LightGBM的HXMT在轨运行模式监测算法

HXMT卫星的空间硬X射线巡天和定点观测计划切换频繁,需要对卫星有效载荷在轨状态进行实时监测和判别.目前采用的是地面监测人员根据总结的规则进行人工监测的方式,虽然执行方便,可解释性强,但人力消耗较大,且对规则之外的情况无法灵活处理.本文利用HXMT卫星的实时遥测数据,提出一种基于LightGBM机器学习模型的在轨运行模式监测算法,将监测工作规约为多分类问题,并构建判别模型,对卫星在轨运行模式进行判断.在保障判别准确率的前提下,算法模型构建迅速,具有很高的实用性.基于真实遥测数据的试验表明,模型的判别准确率达到99.9%,满足在轨运行模式监测要求,可为HXMT卫星的运行监控任务提供参考依据.      

Status of the Hard X-ray Modulation Telescope Project

The Hard X-ray Modulation Telescope (HXMT) is China's first astronomical satellite. It will perform a broad band (1-250keV) scan survey and do pointed observations of X-ray sources to study their spectra and multi-wavelength temporal properties. The pre-flight models of the satellites have been finished, and the flight models are in production. The expected launch date of HXMT is in late 2015.      

HXMT卫星长期任务规划算法

硬X射线调制望远镜（HXMT）卫星是中国首颗空间X射线天文卫星.为充分利用卫星资源,使科学产出最大化,需要进行长期任务规划.长期任务规划是一个复杂的多目标优化问题.通过分析HXMT观测特点和约束条件,建立了HXMT长期任务规划问题模型,并采用贪婪算法加遗传算法对模型进行求解.实例分析结果表明该方法能够有效解决HXMT长期任务规划问题.      

Status of the Hard X-ray Modulation Telescope Project

The Hard X-ray Modulation Telescope (HXMT) is China's first X-ray (1-250 keV) astronomical satellite officially approved in 2011. It will scan the Galactic plane to detect new transient sources and do pointed observations of X-ray sources to study their spectra and multiwavelength temporal properties. Now the flight model of the satellite is in the final testing stage, and the expected launch date is in late 2016.      

HXMT satellite for space hard X-ray observation

In this paper, the Hard X-ray Modulation Telescope mission is introduced. Its primary objective is to perform the hard X-ray all sky survey of high resolution and high sensitivity. The expected angular resolution and position accuracy of the satellite are better than 10^′ and 2^′, respectively. The preliminary mission design is analyzed. And a new attitude subsystem scheme is presented to meet the high precision demand of attitude determination. A conclusion is drawn that the mission design is feasible. The possible launch of it will significantly advance the astrophysical study.     

硬X射线调制望远镜(HXMT)天文卫星的结构分析

根据HXMT卫星的结构形式,建立卫星的有限元模型,进行静力、模态、频率响应计算,得出了最大纵向、最大横向过载联合作用下卫星各组成部分的最大应力值.对整星结构进行了模态计算和频率响应分析,得出了100Hz以内的模态频率值.结合理论分析和以往的设计经验,提出了对该卫星结构的合理改进建议.      

HXMT卫星快视成像

硬X射线调制望远镜(Hard X-ray Modulation Telescope,HXMT)的最重要的工作模式是扫描观测,包括巡天扫描观测和小天区深度扫描观测. HXMT的标准成像需要被观测天区完整的二维扫描观测数据,而同时利用HXMT的观测数据中包含的空间调制信息和旋转调制信息,快视成像可以在只有一维扫描的情况下获得被观测天区的较粗略的流强分布,从而可以在卫星的视场扫过一块天区后很快给出被观测天区的尽可能多的信息.本文详细介绍了快视成像的过程,并通过模拟计算给出了巡天扫描观测快视成像的灵敏度、定位精度和角分辨能力的分布.快视成像能提高HXMT发现暂现源的灵敏度,及时发现并定位出现在HXMT视场中的高能爆发现象,减少较强的暂现源和爆发对标准成像干扰将是标准成像的重要补充.      

The HESP/R satellite project

The aim of the HESP/R (High Energy Solar Physics/Radiation) satellite project is to obtain data of γ-ray, hard X-ray soft X-ray, EUV, and visible radiation of solar flares at the next solar maximum in order to study physics of flares. The HESP/R will be a spinning satellite of 4–5 rotations per min., and the spin axis is off-set by a small angle (0.5°–1.0°) from the Sun. Total weight will be 400 kg and launched in 1991 with M-3S-II rocket by ISAS.     

Physics of the impulsive phase of solar flares

The physics of the impulsive phase of solar flares is discussed in relation to high resolution microwave, hard X-ray and ultraviolet observations. High spatial resolution observations of the structure of microwave flaring loops and their interpretation in terms of arcades of loops as the sites of primary energy release are presented. Theoretical interpretation of the confinement of microwave producing energetic electrons in the coronal part of loops is discussed. High temporal and spatial resolution measurements in hard X-rays, as well as observations of the spectral evolution of the hard X-ray emission are presented. Observations of the relative locations of microwave and hard X-ray emitting regions are presented and their significance with respect to the energy release site and electron acceleration is discussed. The relative timing of the peaks of impulsive hard X-ray and microwave burst is discussed. The significance of ultraviolet measurements in obtaining the density of flaring regions is discussed. Possible diagnostics of impulsive phase onsets from cm-λ polarization data are presented, and the role of the emergence of new flux and of the current sheet formed between closed loops in producing impulsive energy release at centimeter wavelengths are analyzed. Decimeter and meter wave manifestations of preflash phase and millisecond pulsations at centimeter and decimeter wavelengths and the relevant physical processes involved are discussed.     

X-ray imaging techniques— modulation collimator and coded mask

Imaging over the hard X-ray energy band may be achieved by masking the flux with proper obstacles. The imaging modulation collimator has been developed and has been applied thus far, e.g., to produce hard X-ray pictures of the solar flare and to construct the X-ray image of the Crab Nebula up to the angular resolution of ～ 10 arcsec. Variations of the concept such as the Fourier Transform Telescope are discussed. Virtue of the modulation collimator is that high angular resolution may be achieved with a relatively simple detector system and that a wide field of view may be accomodated. Among several proposed coded masks, the techniques of Hadamard transform are discussed in some details. The coded mask is provided with a better total transmission, but its angular resolution is limited due to presently limited spatial resolution of the detector. Developments of the technique of the position sensitive detector are awaited for further improvements of the resolution.     

A method in near-surface estimation of air temperature (NEAT) in times following the satellite passing time using MODIS images

Air temperature is one of the most important parameters in environmental, agricultural and water resources studies. This information is not usually always available at the required temporal and spatial resolution. The air temperature is measured at a fixed point in the meteorological stations which are dispersed and may not have the appropriate spatial resolution needed for many applications. On the other hand, MODIS satellite images have relatively acceptable spatial resolution specially for use in environmental studies. There is a methodology with which the near surface air temperature can be extracted from MODIS images at the satellite passing time with an acceptable accuracy. The goal in this study is to find a way to predict the air temperature in times after/before the satellite passing time. The procedure consists of two steps. In the first step, the relationship between the air temperature at a time in a synoptic station and the air temperature in other times up to 5 h later were modeled. In the second step, using these built up relationships, the air temperature extracted from the satellite image at the passing time was extrapolated to the next hours. Finally, the results of this extrapolation method were evaluated using the air temperatures measured at those hours and in the pixels containing some other meteorological stations. The error of the method when applied to a relatively homogeneous surface cover was about 1.5 °C. This error when applied to the next hours, was below 2 °C up to 5 h after satellite passing time. This method can be useful in some agricultural and horticultural applications in which both the spatial and temporal resolution are needed simultaneously. This product is a useful tool for frost prediction, a phenomenon that usually happens at night or early in the morning.     

太阳微波爆发精细结构与硬X射线耀斑的相关

北京天文台在２．８４ＧＨｚ频率上观测到的带短时标精细结构的微波爆发与日本ＹＯＨＫＯＨ卫星上ＨＸＴ在１９９１年１０月－１９９２年１２月观测到的硬Ｘ射线爆发（ＨＸＢ）事件作了比较，发现在２０个微波精细结构爆发事件只有１２个与ＹＯＨＫＯＨ卫星记录的ＨＸＢ有对应关系．本文对１９９２年６月７日典型事件中２．８４ＧＨｚ与ＨＸＢ共同存在的百秒量级的准周期振荡作了分析及源区参数的计算，并作了简要的讨论．     

High Energy X-ray Telescope Data Analysis Method

The science analysis of the data from the High Energy X-ray Telescope （HE） on the Hard X-ray Modulation Telescope （HXMT） satellite is organized in three stages: calibration, screening and extraction of high-level scientific products. At the first stage, the raw PHA value of each event is converted to PI value accounting for temporal changes in gain and energy offset. At the second stage, the calibrated events are screened by applying cleaning criteria. At the third stage, scientific products, i.e. spectra, light curves and redistribution matrix files, are extracted. This work will introduce the three stages as well as the screening criteria and the data combining method.      

Solar maximum mission experiment: Early results of the hard X-ray imaging experiment

We have selected four widely different flares from the early period of operations of the Hard X-Ray Imaging Spectrometer (HXIS) on SMM to illustrate the characteristic imaging properties of this experiment. For the small flare of April 4, 1980, we demonstrate the instrument's capability for locating a compact source. In the weak, but extensive, flare of April 6 we show how well the instrument can display spatial structure, and also the low level of the instrument background. In the 1B flare of April 7 we are able to locate positions of the X-ray emission in the soft and hard channels, and estimate the positional variations of the emission patches. Finally, in the IN flare of April 10, which produced the strongest hard X-ray burst we have seen so far, we repeat some of the studies made for the April 7 event, and also demonstrate the capability of the HXIS instrument to study the development, with high time resolution, of individual 8″ × 8″ elements of the flare.     

FY-2卫星的空间环境数据接收及警报系统

介绍了FY—2卫星探测数据的流通过程及接收处理．首先在FY-2卫星及探测器系统中，环境探测数据被收集、调制并发射，再由地基数据接收及解调系统将数据信号放大、解调还原并发送，最后由数据处理及警报系统将数据接收处理、保存显示，并对太阳质子事件、x耀斑进行自动电话报警．该系统是保障航天器安全和提高抗辐照水平的重要手段．     

HXMT卫星空间环境监测器及初步观测结果

硬X射线调制望远镜（HXMT）卫星是中国首个专门进行天文探测的空间科学实验卫星,运行于高度约550km、倾角约43°的低地球轨道.星载空间环境监测器为星上科学任务开展提供背景辐射实测资料.该监测器采用固体探测器望远镜系统和扇形阵列全新组合设计,可获取轨道空间高能质子和高能电子能谱、方向综合动态结果,给出更为全面的粒子辐射分布图像.初步探测结果显示,卫星运行轨道遭遇的带电粒子辐射集中分布在经度80°W-20°E,纬度0°-40°S的南大西洋异常区,粒子辐射在该区域表现出不同程度的方向差异分布,高能电子方向差异分布显著强于高能质子.2017年9月空间环境扰动期间,爆发的太阳质子事件并未对该轨道粒子辐射产生影响,而地磁活动导致该轨道穿越经度120°W-60°E,纬度40°-43°N的北美上空和经度60°-120°E,纬度43°-40°S的澳大利亚西南区域时遭遇增强粒子辐射影响,增强的粒子辐射表现出极强的方向分布.      

Dissipative structure and weak turbulence in the solar corona

We have analysed, for the first time, the high resolution X-ray images of the solar corona, obtained by the Yohkoh Mission, as non-linear extended systems. To quantify the spatio-temporal complexity in this extended system, we use an asymmetric spatial fragmentation parameter computed from a matrix representing an image. Choosing different spatial scales on the same image, wave numbers are computed from the intensity contours and this yields a fragmentation spectrum. This spectrum is used to analyze the images of a complex transient event obtained by the Soft X-ray Telescope board the Yohkoh satellite. The dynamics of the fine structures of the contours suggests the origin of the observed fragmentation to be localized weak turbulence process occuring in an evolving coronal active region.     

MONITORING OF ENERGETIC PARTICLE ENVIRONMENT INSIDE THE CHINA-BRAZIL EARTH RESOURCE SATELLITE

On 14 October 1999, the Chinese-Brazil earth resource satellite (CBERS-1) was launched in China. On board of the satellite there was an instrument designed at Peking University to detect the energetic particle radiation inside the satellite so the radiation fluxes of energetic particles in the cabin can be monitored continuously. Inside a satellite cabin, radiation environment consists of ether penetrated energetic particles or secondary radiation from satellite materials due to the interactions with primary cosmic rays.Purpose of the detectors are twofold, to monitor the particle radiation in the cabin and also to study the space radiation environment The data can be used to study the radiation environment and their effects on the electronics inside the satelhte cabin. On the other hand, the data are useful in study of geo-space energetic particle events such as solar proton events, particle precipitation and variations of the radiation belt since there should be some correlation between the radiation situation inside and outside the satellite.The instrument consists of two semi-conductor detectors for protons and electrons respectively. Each detector has two channels of energy ranges. They are 0.5-2MeV and ≥2MeV for electrons and 5-30MeV and 30-60MeV for protons. Counting rate for all channels are up to 104/(cm2@s)and power consumption is about 2.5 W. There are also the additional functions of CMOS TID (total integrated dose) effect and direct SEU monitoring. The data of CBMC was first sent back on Oct. 17 1999 and it's almost three years from then on. The detector has been working normally and the quality of data is good.The preliminary results of data analysis of CBMC not only reveal the effects of polar particle precipitation and radiation belt on radiation environment inside a satellite, but also show some important features of the geo-space energetic particle radiation.As one of the most important parameters of space weather, the energetic charged particles have great influences on space activities and ground tech nology. CBMC is perhaps the first long-term on-board special equipment to monitor the energetic particle radiation environment inside the satellite and the data it accnmulated are very useful in both satellite designing and space research.     

The Neupert effect and new RHESSI measures of thetotal energy in electrons accelerated in solar flares

It is believed that a large fraction of the total energy released in a solar flare goes initially into acceleratedelectrons. These electrons generate the observed hard X-ray bremsstrahlung as they lose most of their energy by coulomb collisions in the lower corona and chromosphere. Results from the Solar Maximum Mission showed that there may be even more energy in accelerated electrons with energies above 25 keV than in the soft X-ray emitting thermal plasma. If this is the case, it is difficult to understand why the Neupert Effect — the empirical result that for many flares the time integral of the hard X-ray emission closely matches the temporal variation of the soft X-ray emission — is not more clearly observed in many flares. From recent studies, it appears that the fraction of the released energy going into accelerated electrons is lower, on average, for smaller flares than for larger flares. Also, from relative timing differences, about 25% of all flares are inconsistent with the Neupert Effect. The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) is uniquely capable of investigating the Neupert Effec since it covers soft X-rays down to 3 keV (when both attenuators are out of the field of view) and hard X-rays with keV energy resolution, arcsecond-class angular resolution, and sub-second time resolution. When combined with the anticipated observations from the Soft X-ray Imager on the next GOES satellite, these observations will provide us with the ability to track the Neupert Effect in space and time and learn more about the relation between plasma heating and particle acceleration. The early results from RHESSI show that the electron spectrum extends down to as low as 10 keV in many flares, thus increasing the total energy estimates of the accelerated electrons by an order of magnitude or more compared with the SMM values. This combined with the possible effects of filling factors smaller than unity for the soft X-ray plasma suggest that there is significantly more energy in nonthermal electrons than in the soft X-ray emitting plasma in many flares.